A born-again star, which following a LTP/VLTP becomes an AGB star again, ejects a mass of \(\approx 10^{-4}-10^{-3}\)  (but the mass can be larger even) in a clumpy morphology (e.g., [1]} for a discussion and references).
[2]} model the born-again phase with a duration of 20 years, a wind velocity of \(20 {~\rm km}{~\rm s}^{-1}\) , and a mass loss rate of \(10^{-4} M_\odot {~\rm yr}^{-1}\) .
Following these studies and others, I take a typical ejecta of a born-again star to be clumpy (e.g., [3]}, [4]}, [5]}), to contain a mass of \(\approx 10^{-4} - 10^{-3} M_\odot \) , and to expand at \({\rm few} \times 10 {~\rm km}{~\rm s}^{-1}\) . However, for the inner and slowest parts of the ejecta I take a velocity of \(\simeq 10 {~\rm km}{~\rm s}^{-1}\) .
